Results of the Search for Ultra High-Energy Neutrinos with ANITA-II
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1 Results of the Search for Ultra High-Energy Neutrinos with ANITA-II Abby Goodhue Vieregg for the ANITA Collaboration University of California, Los Angeles 25 March 2010 (ANITA-II Launch Day in Antarctica) A. G. Vieregg, 25 March
2 ANITA Collaboration University of California, Irvine Ohio State University University of Kansas Washington University in St. Louis University of Delaware University of Minnesota University of California, Los Angeles University of Hawaii at Manoa National Taiwan University University College London Jet Propulsion Laboratory Stanford Linear Accelerator Center A. G. Vieregg, 25 March
3 Neutrinos: The Ideal UHE Messenger Photons lost above 100 TeV (pair production on CMB & IR) Protons and Nuclei suffer curvature induced by B fields But: we know there are sources up to ev!! UHE Neutrino Detectors Study: Highest energy observation of extragalactic sources Very distant sources Deep into opaque sources A. G. Vieregg, 25 March
4 Neutrino Production: The GZK Process GZK process: Cosmic ray protons (E> ev) interact with CMB photons A. G. Vieregg, 25 March
5 Neutrino Cross Section Large extra dimensions Weak interaction at E CM not accessible to LHC: 200 TeV GZK nu Std. model L int ~250 km Use Earth-shielding as cross-section analyzer Anchordoqui et al. Astro-ph/ A. G. Vieregg, 25 March
6 Detection Principle: The Askaryan Effect EM shower in dielectric (ice) moving negative charge excess Coherent radio Cherenkov radiation (P ~ E 2 ) if λ > Moliere radius Askaryan Effect Observed with ANITA at SLAC (2006) A. G. Vieregg, 25 March
7 Validation at SLAC ANITA I beamtest at SLAC (June06): proof of Askaryan effect in ice Coherent (P ~ E 2 ) Linearly Polarized A. G. Vieregg, 25 March
8 The ANITA Concept Neutrino signal characteristics: Fast impulse Vertically polarized Ice is radio transparent Large detection volume (1000 km 3 *str) balloon Only top of Cherenkov cone visible RF is vertically polarized! ANITA-II radio Cherenkov 38 km altitude UHE neutrino interaction & particle shower Antarctic Ice Sheet (Lots of ice, radio transparent) A. G. Vieregg, 25 March
9 The ANITA Instrument NASA Long Duration Balloon, launched near McMurdo, Antarctica NASA Solar Panel Array GPS Antenna Array 40 Horn Antennas for Detecting Signal ( MHz) ANITA Instrument Box (computer, signal processing) Bicone antennas for onboard pulsing NASA Science Instrument Package ANITA Solar Panel Array ANITA-I instrument paper: arxiv: [astro-ph] 8 Drop-down antennas (ANITA-II only) Signal direction calculation: basic interferometry Threshold limited by thermal noise A. G. Vieregg, 25 March
10 ANITA-I Results (S. Hoover) Vertical Polarization (neutrino search) Expected Background Observed Events 1 1 Horizontal Polarization (cosmic rays) Expected Background Observed Events 2 16 Radio Synchrotron emission of CR air showers seen! Direction of geo-magnetic field determines polarization direction (F = qv x B) Mostly Hpol in Antarctica CR Energy: order ev, work in progress Measured V pol Vpkpk (mv / m) Measured Polarization (Proxy) Measured vs. Expected Vpol Content χ 2 / ndf / 15 Slope ± A. G. Vieregg, 25 March 2010 Expected V pol Vpkpk (mv 10 / m) Expected Polarization (Proxy)
11 Improvements for ANITA-II ANITA I flight path (K. Palladino) Lower Energy Threshold (x 3 events) Reduce front-end amplifier temp (20%) Improve neutrino trigger efficiency (30%) 8 more antennas (30%) Increased Exposure (x 2 events) Directional trigger masking (30%) Better flight path & more livetime (x 2) ANITA II flight path (R. Nichol) Total improvement: > 5 in neutrino event rate But: reduction in cosmic ray event rate (new trigger) A. G. Vieregg, 25 March
12 ANITA-II Flight 31 day flight Launched: Dec 21 st M events A. G. Vieregg, 25 March
13 Ground Calibration ~115,000 Calibration impulses from a remote field site during flight. Critical for analysis! (R. Nichol) A. G. Vieregg, 25 March
14 Pointing Events to the Ground Elevation angle from horizontal Making an Interferometric Image: Payload Azimuth Angle Pointing Resolution (Calibration Pulser Event) cross-correlate antenna waveforms use timing delay given by direction sum over the whole payload A. G. Vieregg, 25 March
15 Blind Analysis Plan 2 methods of blinding Hidden signal box Event insertion Set cuts on sidebands Estimate background and efficiency Open hidden box, remove inserted events Separate HPol (cosmic rays) from VPol (neutrinos) A. G. Vieregg, 25 March
16 Lots of Man-Made & Thermal Noise Thermal image using all ANITA-II triggers 99% of events are thermal noise Main cut: size of peak of interferometric image Hot-spot veto for neutrinos South Pole Station McMurdo Station A. G. Vieregg, 25 March
17 Separation from Man-Made Events 300k events pass thermal cuts Cluster with: Other events Known bases of activity Hot-Spots Neutrinos are single, isolated events! A. G. Vieregg, 25 March
18 Cluster Multiplicity Estimate man-made background using cluster multiplicities, polarization information, and distributions from bases Signal Region (Blind) A. G. Vieregg, 25 March
19 Unblinding 0.96 Neutrino Bin Cosmic Ray Bin Background Estimate (Thermal + Man-made): 0.61 Analysis Efficiency V Pol (neutrino): / events H Pol (cosmic ray) : / events A. G. Vieregg, 25 March
20 Candidate Events 3 H Pol 2 V Pol 3 HPol events consistent with cosmic rays seen by ANITA-I! Example waveform: Electric Field (mv/m) mv/m Time (ns) Time (ns) A. G. Vieregg, 25 March
21 Cosmic Ray Sky Map AGN (Approximate Cosmic Ray Acceptance Band Shown) ANITA-I CR Neutrino Candidate ANITA-II CR A. G. Vieregg, 25 March
22 Neutrino Candidates A. G. Vieregg, 25 March
23 New Limit on the UHE Neutrino Flux 2 events on a background of / (Feldman-Cousins 90% CL) Paper Submitted to PRL! arxiv: A. G. Vieregg, 25 March
24 The Future: ANITA-III Proposal for flight this week! Improve to over 100 UHECR events Factor of 2 more sensitivity for neutrinos possible A. G. Vieregg, 25 March
25 Summary 2 Neutrino Candidates on a background of / Set new constraints on flux of UHE neutrinos 3 cosmic ray events seen On the edge of seeing cosmogenic UHE neutrinos? ANITA-III will find out! A. G. Vieregg, 25 March
26 A. G. Vieregg, 25 March
27 Separation from Thermal Noise Rejection of Thermal Noise Sample (Upward Pointing Events) 99% of triggers are thermal noise Cut Location Main cut: peak value of the interferometric image and waveform envelope Allow 0.5 background events (from 21M triggers) Efficiency on Calibration Events Cut Value Cut Value A. G. Vieregg, 25 March
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